1. CLASH SZE Observations and Collaborations Keiichi Umetsu, Academia Sinica IAA (ASIAA), Taiwan (September 20, 2010)

2. Contents 1)Thermal Sunyaev-Zel’dovich Effect (tSZE) 2)SZE Importance in Cluster Science 3)Ground-based SZE Instruments 4)“CLASH SZE” Collaborations 5)Weak lensing distortion (shear) + depletion (magnification bias) with Subaru CLASH-SZE wiki CLASH-SZE wiki https://sites.google.com/site/clashsze/

3. 1. Thermal Sunyaev-Zel’dovich Effect (tSZE) Zel’dovich & Sunyaev (1969); Sunyaev & Zel’dovich (1972) Observer CMB Last Scattering surface (z~1100) Hot gas Hot gas with the electron temperature T e >>T CMB (z) Degree of Comptonization: y = (optical depth of gas) x (gain per scattering) = (thermal electron pressure) x (dlos) g =-2 ( =0), g n <0 ( <~220GHz), g =0 ( ~220GHz), g >0 ( >~220GHz) T e -dependent relativistic correction needed for hot clusters (>5% at 90GHz for >8keV clusters) Energy transfer by IC scattering 10^-4 10^-2 10^-2

4. SZE Frequency Spectrum: Theory vs. Measurements Nord et al. 2009, A&A, 506, 623 Abell 2163 (z=0.201) SZE Brightness Relativistic correction: Te=14, 12, 10, 8keV from top to bottom

5. SZE Importance ① Independent of D(z) i.e., free from cosmological brightness dimming, Power of tSZE: tSZE brightness is ② A measure of projected thermal electron pressure Complementary to X-ray Bremsstrahlung Inverse Compton (no redshift dimming) AMiBA-7 SZE images (Wu et al. 2009, ApJ, 694, 1619)

6. 2. Science with SZE+ CosmologyCosmology –Cluster counts and evolution, N(z) –SZE power spectrum (  8) –Hubble diagram by SZE+X (0.18<z<0.9) Cluster PhysicsCluster Physics –Total thermal energy Gas mass fractions, f gas (r), from lensing+X+SZE Thermal pressure, P gas (r): universal? equilibrium? Entropy profile shapes (Tozzi & Norman ’01; Cavaliere+05) Mass proxy: Y-M and deviations –IC gas structure Merger shocks and substructure –Greater frequency of violent activities at z> (  m /  DE )^(1/3w)-1 ~ 0.4 Gas clumpiness Accretion shocks in cluster outskirts (ALMA) –Gas radial velocities (w.r.t. CMB) by kinematic SZE Sensitive multifrequency SZE, including 220GHz needed (Planck) Higher resolution, sensitivity

7. Science Highlight (I): Baryon Fractions Umetsu, Birkinshaw, Liu et al. 2009, ApJ, 694, 1643 (arXiv:0810.969) Komatsu et al. 2010, WMAP-7yr WMAP7 tSZE and X-ray constraints AMiBA-7 tSZE + WL + X-ray Large-scale f gas constraints (~0.8r vir, =0.2) from tSZE+WL+X, independent of dynamical state and level of hydrostatic equilibrium Vikhlinin+2009

8. Science Highlight (2): Level of H.E. Level of Hydrostatic Equilibrium (H.E.) in relaxed clusters Level of Hydrostatic Equilibrium (H.E.) in relaxed clusters : Thermal (hot gas) to equilibrium (lensing) pressure ratio in clusters? Theory Theory: Molnar, Chiu, Umetsu+10 AMR1: relaxed AMR2: relaxed AMR3: disturbed Nonthermal pressure contribution in relaxed (high-mass) clusters takes a minimum of ~15% at 0.1R vir, growing to >30% at r=R vir. (cf. Lau, Kravtsov, Nagai 09). Subsonic random gas motions at r<0.1R vir contributes by 15%-40% M>1e15 Msun Observations Observations: Kawaharada, Okabe, Umetsu+10 Suzaku-Xray on A1689 Thermal to equilibrium pressure ratio

9. Methodology: (X+SZE) + Lensing Detailed X+SZE modeling of (n, T)Detailed X+SZE modeling of (n, T) (e.g., Molnar, Umetsu, Birkinshaw+10, ApJ, arXiv:1009.1943) –Calibrated by high-resolution cosmological simulations –High-resolution X-ay data to constrain the central structure parameters of (n, T) typically at r<r 500 –Large-scale SZE (e.g., AMiBA) to constrain the normalization and outer scale of P(r) typically at r~r 200 Simultaneous X+SZE deprojection of (n, T)Simultaneous X+SZE deprojection of (n, T) (e.g., Ameglio+07, MNRAS, 382, 397; Nord+09, A&A, 506, 623) –Non-parametric –Spherical symmetry assumed –Without using spectroscopic X-ray temperature (cf. Mazzotta+04) Lensing data to constrain the total massLensing data to constrain the total mass –Free from any equilibrium assumption (Umetsu+09; Zhang+10)

10. Non-Parametric X+SZE Deprojetion Joint Abel deprojection Joint Abel deprojection (Silk & White 1978) Color-coded: APEX-SZ APEX-SZ (150GHz) XMM-Newton Contours: XMM-Newton A2163 (z=0.21): Nord et al. (2009)

11. SZE-dedicated - Bolometers: ACT (145,225,265 GHz), APEX-SZ (150,217 GHz), SPT (95,150,225 GHz) - Interferometers: AMI (15GHz), AMiBA (90GHz), SZA (30,90GHz) General purposes - Bolometers: GBT/MUSTANG @90GHz, Bolocam @150GHz - Interferometers: CARMA-SZA @30,90GHz - Single dish radiometer: OCRA @30GHz Blue: multi-pixel bolometer array Red: interferometer array Green: single dish radiometer 3. Ground-based SZE Instruments

12. SZE Frequency Coverage SPT ACT APEX Bolocam SZA (BIMA,CBI, VSA) Red: Interferometer Blue: Multi-pixel bolometer primary CMBforeground emission – Relative SZE strength w.r.t. primary CMB and foreground emission is maximized at 90- 100GHz. – CMB/SZE interferometers based on HEMT (<100GHz). – Except CSO/Bolocam (+19.8d) and GBT/Mustang (+38.4d), SZE bolometers are mostly sited in the southern hemisphere. SPT ACT APEX AMiBA [SZA] SPT, GBT/Mustang AMI Figure from Zhang+02

13. 4. CLASH-SZE Collaborations CLASH-SZE –Collaboration between CLASH and several groups observing the SZ effect (Bolocam, Mustang, AMiBA, SZA) –CLASH-SZE wiki –CLASH-SZE wiki has been set up thanks to Dan https://sites.google.com/site/clashsze/ Rationale: Rationale: SZE counter part of “ACS+Subaru” multiscale lensing collaboration –Large scale SZE –Large scale SZE (1’-10’) Bolocam@150GHz (8’ FoV, 1’ res) AMiBA-13@94GHz (11’ FoV, 2’ res) or (22’ FoV, 3’ res) SZA@30GHz (11’ FoV, 1’ res) –Small scale SZE –Small scale SZE (10”-1’) GBT/Mustang@90GHz (40”x40” FoV, 9” res) SZA@90GHz (4’ FoV, 20” res) Two-types of collaboration involved Two-types of collaboration involved: –CLASH lensing+SZE+ collaboration (involving CLASH data) –Multiscale SZE collaboration (pure SZE collaboration)

14. (1) CLASH-Bolocam SZE Collaboration 12 nights proposed for 2010B in collaboration with the Bolocam team: 14 nights allocated!! Umetsu/National, Golwala/Caltech, Moustakas/JPL  14 nights allocated!! Observers Bolocam SZE observations in October 8-21 (Observers: K. Umetsu, P. Koch, S. Molnar, K.-Y. Lin, J. Sayers, N. Czakon) Status Summary Status Summary: 12/25 CLASH clusters observed with by the Bolocam team+ 8 clusters TBO in 2010B+2011A with CLASH+Bolocam collaboration 5 clusters in accessible from MK Figures by Sunil Golwala, Jack Sayers+

15. (2) CLASH-Mustang Collaboration B. Mason et al. 2010 Status Summary Status Summary: 3 CLASH targets observed (CLJ1226+33, MACSJ0744+39, RXJ1347-11) 1 more in fall 2010 (MACSJ0717+37) Planning on joint Mustang proposal with CLASH

16. (3) AMiBA and SZA Interferometers AMiBA-7 (2006-2008) AMiBA-13 (2010-) Sunyaev Zeldovich Array Ho, P.T.P.+2009, ApJ Muchovej, S. et al. 2007, ApJ

17. Summary Mid-term –The baseline of collaboration policies has been set up For papers involving HST-CLASH data, we will invite all of the CLASH core members (those 23 on the HST MCT proposal) to join as co-authors. Each of the SZE groups may have similar policies at their discretion. That is, whenever their data is used, they decide who on their team should be invited to join on the paper. –Details to be discussed further (individually and collectively among the groups) Short-term –Upcoming Mustang proposal: coordination with Brian Mason et al.

18. Distortion vs. Magnification-Bias (Counts) Profiles Count depletion of red background galaxies being consistent with the tangential distortion!!!

19. Bayesian mass profile reconstruction Bayesian analysis of joint distortion and magnification (counts) profiles Model independent Mass-sheet (boundary condition) free Automatically account for the depth miss-match between the distortion (blue+red) and magnification (red) galaxy samples Individual (lines) and stacked (red) surface mass density profiles of 5 massive clusters Model independent constraints on the density slope, d  /dr Preliminary results (Umetsu+2010, in prep)

20. Sample of Cluster Mass Profiles Distortion + Magnification Umetsu+2010 in prep

21. Fin

22. Appendix: Foreground Contaminations Synchrotron Dust Typical SEDs of Galaxies – most radio point sources have negative spectral index CMB interferometers: CBI (@30GHz) AMI (@15GHz) SZA (@30/90GHz)

23. Appendix: SZE with ALMA